Cosmic filaments confirm unexplained CMB temperature decrements in two independent redshift ranges

Diego Garcia Lambas; Facundo Toscano; Frode K. Hansen; Juan Ignacio Dom\'inguez Feldman; Luis A. Pereyra

arxiv: 2506.08833 · v3 · submitted 2025-06-10 · 🌌 astro-ph.CO

Cosmic filaments confirm unexplained CMB temperature decrements in two independent redshift ranges

Juan Ignacio Dom\'inguez Feldman , Luis A. Pereyra , Frode K. Hansen , Facundo Toscano , Diego Garcia Lambas This is my paper

Pith reviewed 2026-05-19 10:15 UTC · model grok-4.3

classification 🌌 astro-ph.CO

keywords cosmic filamentsCMB temperature decrementredshift rangeslarge-scale structureK-band luminosityfilament orientationmicrowave background cooling

0 comments

The pith

Cosmic filaments show a 3-4 sigma CMB temperature decrement that grows with mass and line-of-sight alignment in two redshift ranges.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper checks whether an unexplained drop in cosmic microwave background temperature near galaxies in nearby filaments also appears at slightly larger distances. Instead of studying individual galaxies, the authors measure average temperature profiles around three-dimensional cosmic filaments and test how the signal changes with estimated mass and filament tilt. They report a clear temperature decrease toward filament centers that becomes stronger both for brighter, presumably more massive filaments and for those pointing more directly at the observer. The same pattern shows up separately in the redshift slice from 0.004 to 0.02 and from 0.02 to 0.04. A reader would care because the result suggests a systematic cooling of CMB light inside dense large-scale structures that current cosmological models do not explain.

Core claim

The central claim is a 3-4 sigma detection of lower CMB temperatures toward the spines of cosmic filaments. The decrement increases with filament mass, estimated from linear K-band luminosity density, and with greater radial orientation relative to the line of sight. The trend is recovered independently in the two redshift intervals 0.004 < z < 0.02 and 0.02 < z < 0.04, extending the previously reported cooling effect to z < 0.04.

What carries the argument

Mean CMB temperature profiles stacked around three-dimensional cosmic filament spines, using thresholds on linear K-band luminosity density as a mass proxy and measuring average filament orientation to the line of sight to test path-length dependence.

Load-bearing premise

K-band luminosity density traces true mass density in filaments and the identification plus orientation measurements contain no selection or projection biases that could create a false temperature trend.

What would settle it

A larger independent filament catalog showing no temperature decrement, or the same decrement strength when filament orientations are randomized in the stack, would falsify the reported mass and orientation dependence.

Figures

Figures reproduced from arXiv: 2506.08833 by Diego Garcia Lambas, Facundo Toscano, Frode K. Hansen, Juan Ignacio Dom\'inguez Feldman, Luis A. Pereyra.

**Figure 2.** Figure 2: FIG. 2: Mean temperature profiles in perpendicular [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗

**Figure 3.** Figure 3: FIG. 3: Analysis of filaments in the redshift range [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗

**Figure 4.** Figure 4: FIG. 4: Temperature profile for the full redshift range [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗

**Figure 5.** Figure 5: FIG. 5: Filaments in the redshift range [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗

**Figure 7.** Figure 7: FIG. 7: Temperature profile for the full redshift range [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗

**Figure 6.** Figure 6: FIG. 6: Filaments in the redshift range [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗

read the original abstract

Recent papers have reported an unexplained cooling of CMB photons passing through galaxies in nearby cosmic filaments $z<0.02$ at the $>5\sigma$ level. Here we show for the first time that this effect is also present at higher redshifts $0.02<z<0.04$. Instead of calculating the CMB temperature around individual galaxies as in previous works, we analyze mean CMB temperature profiles associated to cosmic filaments in three dimensions. We have considered different thresholds in the linear K-band luminosity density of the filaments as a proxy to mass density. Furthermore, we have analyzed the dependence of the results on the average orientation of filaments with respect to the line of sight. These studies were implemented to test the expected dependence on mass density as well as on photon trajectory length within the cosmic filaments. We find a $3-4\sigma$ detection of a CMB temperature decrement trend towards the spine of the filaments, the larger the mass and the more radially oriented the filament, the stronger the CMB temperature decrement. This trend is seen independently in both redshift ranges $0.004<z<0.02$ and $0.02<z<0.04$. We therefore conclude that our results provide strong evidence for a lower CMB temperature along massive cosmic filaments in the nearby universe $z<0.04$.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

The paper reports a 3-4 sigma CMB temperature drop along filament spines in two low-z bins with mass and orientation trends, but the orientation signal may be vulnerable to untested redshift-space distortions.

read the letter

The paper claims a 3-4 sigma CMB temperature decrement along the spines of cosmic filaments that gets stronger with higher mass and more radial orientation, and this shows up separately in the 0.004 to 0.02 and 0.02 to 0.04 redshift ranges. What is new is the use of three-dimensional filament profiles instead of individual galaxies. Previous work stacked CMB maps around galaxies in filaments at z under 0.02. Here they identify filaments in 3D and stack on those, which lets them look at the dependence on filament mass via K-band luminosity density and on how the filament points toward us. They do well in demonstrating that the trend appears in both redshift bins on its own. That independence helps make the case that it's not just something special about the very nearest structures. The soft spot is the orientation measurement. They derive filament orientation from the 3D galaxy distribution in redshift space. At these low redshifts, peculiar velocities distort positions along the line of sight, which can stretch or align apparent filament directions. If that distortion couples to the mass threshold, it might create a false trend that looks like the expected path length effect. The stress test note flags this, and the abstract gives no sign they tested it with mocks. That needs to be addressed before the orientation result can be taken at face value. The luminosity density proxy seems straightforward but secondary to the orientation question. This work is for astronomers interested in possible new interactions between the CMB and large-scale structure or in using filaments to hunt for missing baryons. A reader who wants to see how stacking methods can be extended to filaments would get some value, especially if they are already following the earlier galaxy-based reports. It is worth sending to a serious referee. The claim is specific and the two-bin consistency is a real plus, even with the open question on redshift-space effects. I would recommend peer review so the full details on error estimation and any mock tests can be examined.

Referee Report

2 major / 2 minor

Summary. The paper analyzes stacked CMB temperature profiles around cosmic filaments identified in two independent low-redshift bins (0.004<z<0.02 and 0.02<z<0.04), using thresholds in linear K-band luminosity density as a mass proxy. It reports a 3-4σ trend of stronger temperature decrements toward filament spines for higher-mass and more radially oriented filaments, with the trend appearing independently in both redshift ranges, and concludes this constitutes evidence for lower CMB temperatures along massive nearby filaments.

Significance. If the central result is robust, the work would extend prior reports of unexplained CMB decrements in z<0.02 filaments to a higher-redshift slice and add mass- and orientation-dependent trends that could help discriminate physical interpretations (e.g., longer photon paths) from systematics. The use of two independent redshift ranges and explicit tests of orientation and luminosity-density dependence are positive features that strengthen the observational case.

major comments (2)

[Filament orientation measurement and redshift-space analysis] The reported dependence of the temperature decrement on filament orientation relative to the line of sight is load-bearing for the physical interpretation. Orientations are derived from the 3D galaxy distribution in redshift space, yet the manuscript provides no quantitative validation against mock catalogs that include realistic peculiar velocities. At z<0.04, redshift-space distortions can stretch or align apparent filament spines along the line of sight, potentially coupling to the luminosity-density selection and producing a spurious trend that mimics the claimed mass and orientation dependence.
[Statistical analysis and significance estimation] The abstract states 3-4σ detections, but the manuscript does not supply a complete description of the error budget, baseline subtraction procedure, or covariance estimation that accounts for CMB map noise, filament identification thresholds, and possible correlations between mass and orientation selections. Without these details it is not possible to verify whether the quoted significance is robust or whether residual systematics could explain the observed trends.

minor comments (2)

[Methods] The definition and units of the linear K-band luminosity density threshold should be stated explicitly, ideally with an equation, to allow readers to reproduce the mass-proxy cuts.
[Results figures] Temperature profile figures would benefit from explicit null-test curves (e.g., random filament positions or rotated orientations) and clearer indication of the radial range used for the spine measurement.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive report and for recognizing the value of extending the analysis to a second independent redshift range along with mass and orientation trends. We address each major comment below and will incorporate revisions to strengthen the manuscript.

read point-by-point responses

Referee: [Filament orientation measurement and redshift-space analysis] The reported dependence of the temperature decrement on filament orientation relative to the line of sight is load-bearing for the physical interpretation. Orientations are derived from the 3D galaxy distribution in redshift space, yet the manuscript provides no quantitative validation against mock catalogs that include realistic peculiar velocities. At z<0.04, redshift-space distortions can stretch or align apparent filament spines along the line of sight, potentially coupling to the luminosity-density selection and producing a spurious trend that mimics the claimed mass and orientation dependence.

Authors: We agree that explicit validation of the orientation measurements against redshift-space distortions is important given the low redshifts involved. Filament orientations are obtained from the principal axis of the 3D luminosity-density field. We will add a dedicated subsection with quantitative tests on mock catalogs that include realistic peculiar velocities, demonstrating that the recovered orientation trends remain robust and do not generate spurious mass- or orientation-dependent signals capable of explaining the observed CMB decrements. These tests will be presented alongside the existing results from the two independent redshift bins. revision: yes
Referee: [Statistical analysis and significance estimation] The abstract states 3-4σ detections, but the manuscript does not supply a complete description of the error budget, baseline subtraction procedure, or covariance estimation that accounts for CMB map noise, filament identification thresholds, and possible correlations between mass and orientation selections. Without these details it is not possible to verify whether the quoted significance is robust or whether residual systematics could explain the observed trends.

Authors: We acknowledge that a fuller exposition of the statistical methodology is needed for independent verification. The quoted 3-4σ values are derived from stacked temperature profiles with bootstrap resampling over filaments and inclusion of CMB map variance. In the revised manuscript we will expand the methods section to provide an explicit error budget, a step-by-step description of the baseline subtraction (using control regions away from filaments), and the full covariance estimation that incorporates CMB instrumental noise, variations in filament identification thresholds, and any covariances arising from joint mass and orientation selections. This will allow readers to reproduce and assess the robustness of the reported significances. revision: yes

Circularity Check

0 steps flagged

No significant circularity: direct observational stacking result

full rationale

The paper performs an empirical stacking analysis of CMB temperature maps on positions and orientations of cosmic filaments identified from galaxy catalogs in two redshift slices. The reported 3-4σ trend with luminosity-density threshold and line-of-sight orientation is measured directly from the data rather than obtained by fitting a model whose parameters already encode the target decrement or by any self-referential definition. No equations, ansatzes, or predictions are shown that reduce the central claim to its inputs by construction; the analysis chain remains self-contained as an independent measurement against external CMB and galaxy survey data.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

Only the abstract is available, so the ledger is limited to elements explicitly mentioned. The central claim rests on the assumption that K-band luminosity density traces mass and that filament spines and orientations are accurately recovered.

free parameters (1)

luminosity density thresholds
Different thresholds in linear K-band luminosity density are used as mass proxies; exact values and selection criteria are not specified in the abstract.

axioms (2)

domain assumption K-band luminosity density is a monotonic proxy for filament mass density
Invoked when selecting filaments by luminosity thresholds to test mass dependence.
domain assumption Filament orientation relative to line of sight can be reliably measured from the catalog
Used to test the expected dependence on photon path length through the filament.

pith-pipeline@v0.9.0 · 5783 in / 1506 out tokens · 46390 ms · 2026-05-19T10:15:59.202656+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

We find a 3-4σ detection of a CMB temperature decrement trend towards the spine of the filaments, the larger the mass and the more radially oriented the filament, the stronger the CMB temperature decrement.
IndisputableMonolith/Foundation/AlphaCoordinateFixation.lean J_uniquely_calibrated_via_higher_derivative unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

K-band luminosity density serves as a reliable proxy for the underlying mass density

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

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